By using the mass estimation of the secondary component of GW190814 system, in combination with the fitting formulas mentioned above, we obtained estimations on the speed of sound values for each transition density \(n_{\mathrm {tr}}\)  scenario. In particular, for a non-rotating massive neutron star with \(M=2.59\;M_\odot \)  the value of the speed of sound must be (a) \((v_s/c)^2 = 0.485\)  (\(n_{\mathrm {tr}}=1.5n_s\) ), and (b) \((v_s/c)^2 = 0.659\)  (\(n_{\mathrm {tr}}=2n_s\) ). The exact values' interval is given in Table REF . We observe that for higher values of transition density \(n_{\mathrm {tr}}\)  the fitted curve and marks are shifted downwards; hence the higher the point of the transition in density, the smaller the provided maximum mass. The higher values of speed of sound are more suitable to describe such massive neutron stars, until a specific boundary value of transition density \(n_{\mathrm {tr}}\)  in which even the causality would not be suitable. Therefore, a very massive non-rotating neutron star favors higher values of speed of sound than the \(v_s=c/\sqrt{3}\)  limit. We notice that a lower bound on the transition density \(n_{\mathrm {tr}}\)  is needed to be able in the description of the observed neutron star mergers [1]}. Therefore there is a contradiction since the transition density \(n_{\mathrm {tr}}\)  must be above a specific lower limit and not big enough to predict very massive masses. This kind of remark arises in the speed of sound value, respectively.
